All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{h4485f1.eps}\end{figure}$ Figure 1: ISO-SWS spectra of the lines detected in NGC 6240. Some of the ranges from which important upper limits are derived are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{h4485f2.eps}\end{figure}$ Figure 2: Infrared spectral energy distribution of NGC 6240 from ISO observations. Continuous lines show the ISOCAM-CVF and LWS spectra, histograms the ISOPHOT-S spectrum. Small crosses indicate continua from the SWS spectra at > $16~\mu$ m, where the relative zodiacal light contribution is small. Asterisks indicate the broad band photometry of Klaas et al. (1997, 2001).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4485f3.eps} \end{figure}$ Figure 3: Fine-structure emission line ratios for NGC 6240, compared to a number of bright AGN from Sturm et al. (2002), the starbursts of Verma et al. (2003, excluding low metallicity dwarfs), and the supernova remnants IC 443 and RCW 103 (Oliva et al. 1999a,b). The overplotted grid represents simple mixing by a linear superposition of starburst, SNR, and AGN line spectra. The loci of the grid lines indicate where the contribution to [Ne II] is 0%, 10%, 20%, ... for supernova remnants and for AGN. The percentage contribution to other lines will be different. Note that the four leftmost AGN themselves have evidence (PAH emission) for significant star formation inside the SWS beam.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4485f4.eps} \end{figure}$ Figure 4: H₂ excitation diagram for NGC 6240, showing for the lines observed with SWS the upper level population divided by the level degeneracy, as a function of upper level energy. The level populations are derived from observed fluxes without extinction correction.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{h4485f5.eps} \end{figure}$ Figure 5: Low resolution ISOCAM 5-16 $\mu$ m spectrum of NGC 6240 compared to a scaled spectrum of M 82 (top) and a schematic model consisting of the sum of a scaled M 82 spectrum and an absorbed power law continuum (bottom). Obscuration of the continuum is needed for a satisfactory representation including the region of silicate feature. The schematic model is inadequate in the regions of strong emission lines because of differences in the emission line spectra of NGC 6240 and M 82.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{h4485f1.eps}\end{figure}$	Figure 1: ISO-SWS spectra of the lines detected in NGC 6240. Some of the ranges from which important upper limits are derived are also shown.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16cm,clip]{h4485f2.eps}\end{figure}$	Figure 2: Infrared spectral energy distribution of NGC 6240 from ISO observations. Continuous lines show the ISOCAM-CVF and LWS spectra, histograms the ISOPHOT-S spectrum. Small crosses indicate continua from the SWS spectra at > $16~\mu$ m, where the relative zodiacal light contribution is small. Asterisks indicate the broad band photometry of Klaas et al. (1997, 2001).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4485f4.eps} \end{figure}$	Figure 4: H₂ excitation diagram for NGC 6240, showing for the lines observed with SWS the upper level population divided by the level degeneracy, as a function of upper level energy. The level populations are derived from observed fluxes without extinction correction.
Open with DEXTER